@article{SchmollDietrichWinkeletal.2005, author = {Schmoll, Tim and Dietrich, Volkmar and Winkel, Wolfgang and Epplen, J. T. and Schurr, Frank Martin and Lubjuhn, Thomas}, title = {Paternal genetic effects on offspring fitness are context dependent within the extrapair mating system of a socially monogamous passerine}, year = {2005}, abstract = {Avian extrapair mating systems provide an interesting model to assess the role of genetic benefits in the evolution of female multiple mating behavior, as potentially confounding nongenetic benefits of extrapair mate choice are seen to be of minor importance. Genetic benefit models of extrapair mating behavior predict that females engage in extrapair copulations with males of higher genetic quality compared to their social mates, thereby improving offspring reproductive value. The most straightforward test of such good genes models of extrapair mating implies pail-wise comparisons of maternal half-siblings raised in the same environment, which permits direct assessment of Paternal genetic effects oil offspring traits. But genetic benefits of mate choice may be difficult to detect. Furthermore, the extent of genetic benefits (in terms of increased offspring viability or fecundity) may depend oil the environmental context Such that the proposed differences between extrapair offspring (EPO) and within-pair offspring (WPO) only appear under comparatively poor environmental conditions. We tested the hypothesis that genetic benefits of female extrapair mate choice are context dependent by analyzing offspring fitness-related traits in the coal tit (Parus ater) in relation to seasonal variation in environmental conditions. Paternal genetic effects on offspring fitness were context dependent. as shown by a significant interaction effect of differential paternal genetic contribution and offspring hatching date. EPO showed a higher local recruitment probability than their maternal half-siblings if born comparatively late in the season (i.e.. when overall performance had significantly declined), while WPO performed better early in the season. The same general pattern of context dependence was evident when using the number of grandchildren born to a cuckolding female via her female WPO or EPO progeny as the respective fitness measure. However, we were unable to demonstrate that cuckolding females obtained a general genetic fitness benefit from extrapair fertilizations in terms of offspring viability or fecundity. Thus, another type of benefit Could be responsible for maintaining female extrapair mating preferences in the study population. Our results suggest that more than a single selective pressure may have shaped the evolution of female extrapair mating behavior in socially monogamous passerines.}, language = {en} } @misc{MeyerPalkopoulouBalekaetal.2017, author = {Meyer, Matthias and Palkopoulou, Eleftheria and Baleka, Sina Isabelle and Stiller, Mathias and Penkman, Kirsty E. H. and Alt, Kurt W. and Ishida, Yasuko and Mania, Dietrich and Mallick, Swapan and Meijer, Tom and Meller, Harald and Nagel, Sarah and Nickel, Birgit and Ostritz, Sven and Rohland, Nadin and Schauer, Karol and Sch{\"u}ler, Tim and Roca, Alfred L. and Reich, David and Shapiro, Beth and Hofreiter, Michael}, title = {Palaeogenomes of Eurasian straight-tusked elephants challenge the current view of elephant evolution}, series = {Postprints der Universit{\"a}t Potsdam Mathematisch-Naturwissenschaftliche Reihe}, journal = {Postprints der Universit{\"a}t Potsdam Mathematisch-Naturwissenschaftliche Reihe}, number = {790}, issn = {1866-8372}, doi = {10.25932/publishup-44013}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-440139}, pages = {14}, year = {2017}, abstract = {The straight-tusked elephants Palaeoloxodon spp. were widespread across Eurasia during the Pleistocene. Phylogenetic reconstructions using morphological traits have grouped them with Asian elephants (Elephas maximus), and many paleontologists place Palaeoloxodon within Elephas. Here, we report the recovery of full mitochondrial genomes from four and partial nuclear genomes from two P. antiquus fossils. These fossils were collected at two sites in Germany, Neumark-Nord and Weimar-Ehringsdorf, and likely date to interglacial periods similar to 120 and similar to 244 thousand years ago, respectively. Unexpectedly, nuclear and mitochondrial DNA analyses suggest that P. antiquus was a close relative of extant African forest elephants (Loxodonta cyclotis). Species previously referred to Palaeoloxodon are thus most parsimoniously explained as having diverged from the lineage of Loxodonta, indicating that Loxodonta has not been constrained to Africa. Our results demonstrate that the current picture of elephant evolution is in need of substantial revision.}, language = {en} } @article{MeyerPalkopoulouBalekaetal.2017, author = {Meyer, Matthias and Palkopoulou, Eleftheria and Baleka, Sina Isabelle and Stiller, Mathias and Penkman, Kirsty E. H. and Alt, Kurt W. and Ishida, Yasuko and Mania, Dietrich and Mallick, Swapan and Meijer, Tom and Meller, Harald and Nagel, Sarah and Nickel, Birgit and Ostritz, Sven and Rohland, Nadin and Schauer, Karol and Schueler, Tim and Roca, Alfred L. and Reich, David and Shapiro, Beth and Hofreiter, Michael}, title = {Palaeogenomes of Eurasian straight-tusked elephants challenge the current view of elephant evolution}, series = {eLife}, volume = {6}, journal = {eLife}, publisher = {eLife Sciences Publications}, address = {Cambridge}, issn = {2050-084X}, doi = {10.7554/eLife.25413}, pages = {14}, year = {2017}, abstract = {The straight-tusked elephants Palaeoloxodon spp. were widespread across Eurasia during the Pleistocene. Phylogenetic reconstructions using morphological traits have grouped them with Asian elephants (Elephas maximus), and many paleontologists place Palaeoloxodon within Elephas. Here, we report the recovery of full mitochondrial genomes from four and partial nuclear genomes from two P. antiquus fossils. These fossils were collected at two sites in Germany, Neumark-Nord and Weimar-Ehringsdorf, and likely date to interglacial periods similar to 120 and similar to 244 thousand years ago, respectively. Unexpectedly, nuclear and mitochondrial DNA analyses suggest that P. antiquus was a close relative of extant African forest elephants (Loxodonta cyclotis). Species previously referred to Palaeoloxodon are thus most parsimoniously explained as having diverged from the lineage of Loxodonta, indicating that Loxodonta has not been constrained to Africa. Our results demonstrate that the current picture of elephant evolution is in need of substantial revision.}, language = {en} } @article{ChaurasiaDietrichRosswog2021, author = {Chaurasia, Swami Vivekanandji and Dietrich, Tim and Rosswog, Stephan}, title = {Black hole-neutron star simulations with the BAM code}, series = {Physical review : D, Particles, fields, gravitation, and cosmology}, volume = {104}, journal = {Physical review : D, Particles, fields, gravitation, and cosmology}, number = {8}, publisher = {American Physical Society}, address = {Ridge, NY}, issn = {2470-0010}, doi = {10.1103/PhysRevD.104.084010}, pages = {15}, year = {2021}, abstract = {The first detections of black hole-neutron star mergers (GW200105 and GW200115) by the LIGO-Virgo-Kagra Collaboration mark a significant scientific breakthrough. The physical interpretation of pre- and postmerger signals requires careful cross-examination between observational and theoretical modelling results. Here we present the first set of black hole-neutron star simulations that were obtained with the numerical-relativity code BAM. Our initial data are constructed using the public LORENE spectral library, which employs an excision of the black hole interior. BAM, in contrast, uses the moving-puncture gauge for the evolution. Therefore, we need to "stuff" the black hole interior with smooth initial data to evolve the binary system in time. This procedure introduces constraint violations such that the constraint damping properties of the evolution system are essential to increase the accuracy of the simulation and in particular to reduce spurious center-of-mass drifts. Within BAM we evolve the Z4c equations and we compare our gravitational-wave results with those of the SXS collaboration and results obtained with the SACRA code. While we find generally good agreement with the reference solutions and phase differences less than or similar to 0.5 rad at the moment of merger, the absence of a clean convergence order in our simulations does not allow for a proper error quantification. We finally present a set of different initial conditions to explore how the merger of black hole neutron star systems depends on the involved masses, spins, and equations of state.}, language = {en} } @article{AshtonDietrich2022, author = {Ashton, Gregory and Dietrich, Tim}, title = {The use of hypermodels to understand binary neutron star collisions}, series = {Nature astronomy}, volume = {6}, journal = {Nature astronomy}, number = {8}, publisher = {Nature portfolio}, address = {Berlin}, issn = {2397-3366}, doi = {10.1038/s41550-022-01707-x}, pages = {961 -- 967}, year = {2022}, abstract = {Gravitational waves from the collision of binary neutron stars provide a unique opportunity to study the behaviour of supranuclear matter, the fundamental properties of gravity and the cosmic history of our Universe. However, given the complexity of Einstein's field equations, theoretical models that enable source-property inference suffer from systematic uncertainties due to simplifying assumptions. We develop a hypermodel approach to compare and measure the uncertainty of gravitational-wave approximants. Using state-of-the-art models, we apply this new technique to the binary neutron star observations GW170817 and GW190425 and to the sub-threshold candidate GW200311_103121. Our analysis reveals subtle systematic differences (with Bayesian odds of similar to 2) between waveform models. A frequency-dependence study suggests that this may be due to the treatment of the tidal sector. This new technique provides a proving ground for model development and a means to identify waveform systematics in future observing runs where detector improvements will increase the number and clarity of binary neutron star collisions we observe.}, language = {en} } @article{KoelschDietrichUjevicetal.2022, author = {K{\"o}lsch, Maximilian and Dietrich, Tim and Ujevic, Maximiliano and Br{\"u}gmann, Bernd}, title = {Investigating the mass-ratio dependence of the prompt-collapse threshold with numerical-relativity simulations}, series = {Physical review : D, Particles, fields, gravitation, and cosmology}, volume = {106}, journal = {Physical review : D, Particles, fields, gravitation, and cosmology}, number = {4}, publisher = {American Physical Society}, address = {College Park}, issn = {2470-0010}, doi = {10.1103/PhysRevD.106.044026}, pages = {27}, year = {2022}, abstract = {The next observing runs of advanced gravitational-wave detectors will lead to a variety of binary neutron star detections and numerous possibilities for multimessenger observations of binary neutron star systems. In this context a clear understanding of the merger process and the possibility of prompt black hole formation after merger is important, as the amount of ejected material strongly depends on the merger dynamics. These dynamics are primarily affected by the total mass of the binary, however, the mass ratio also influences the postmerger evolution. To determine the effect of the mass ratio, we investigate the parameter space around the prompt-collapse threshold with a new set of fully relativistic simulations. The simulations cover three equations of state and seven mass ratios in the range of 1.0 <= q <= 1.75, with five to seven simulations of binary systems of different total mass in each case. The threshold mass is determined through an empirical relation based on the collapse time, which allows us to investigate effects of the mass ratio on the threshold mass and also on the properties of the remnant system. Furthermore, we model effects of mass ratio and equation of state on tidal parameters of threshold configurations.}, language = {en} } @article{EmmaSchianchiPannaraleetal.2022, author = {Emma, Mattia and Schianchi, Federico and Pannarale, Francesco and Sagun, Violetta and Dietrich, Tim}, title = {Numerical simulations of dark matter admixed neutron star binaries}, series = {Particles}, volume = {5}, journal = {Particles}, number = {3}, publisher = {MDPI}, address = {Basel}, issn = {2571-712X}, doi = {10.3390/particles5030024}, pages = {273 -- 286}, year = {2022}, abstract = {Multi-messenger observations of compact binary mergers provide a new way to constrain the nature of dark matter that may accumulate in and around neutron stars. In this article, we extend the infrastructure of our numerical-relativity code BAM to enable the simulation of neutron stars that contain an additional mirror dark matter component. We perform single star tests to verify our code and the first binary neutron star simulations of this kind. We find that the presence of dark matter reduces the lifetime of the merger remnant and favors a prompt collapse to a black hole. Furthermore, we find differences in the merger time for systems with the same total mass and mass ratio, but different amounts of dark matter. Finally, we find that electromagnetic signals produced by the merger of binary neutron stars admixed with dark matter are very unlikely to be as bright as their dark matter-free counterparts. Given the increased sensitivity of multi-messenger facilities, our analysis gives a new perspective on how to probe the presence of dark matter.}, language = {en} } @article{DudiAdhikariBruegmannetal.2022, author = {Dudi, Reetika and Adhikari, Ananya and Br{\"u}gmann, Bernd and Dietrich, Tim and Hayashi, Kota and Kawaguchi, Kyohei and Kiuchi, Kenta and Kyutoku, Koutarou and Shibata, Masaru and Tichy, Wolfgang}, title = {Investigating GW190425 with numerical-relativity simulations}, series = {Physical review : D, Particles, fields, gravitation, and cosmology}, volume = {106}, journal = {Physical review : D, Particles, fields, gravitation, and cosmology}, number = {8}, publisher = {American Physical Society}, address = {College Park}, issn = {2470-0010}, doi = {10.1103/PhysRevD.106.084039}, pages = {11}, year = {2022}, abstract = {The third observing run of the LIGO-Virgo Collaboration has resulted in many gravitational wave detections, including the binary neutron star merger GW190425. However, none of these events have been accompanied with an electromagnetic transient found during extensive follow-up searches. In this article, we perform new numerical-relativity simulations of binary neutron star and black hole-neutron star systems that have a chirp mass consistent with GW190425. Assuming that the GW190425's sky location was covered with sufficient accuracy during the electromagnetic follow-up searches, we investigate whether the nondetection of the kilonova is compatible with the source parameters estimated through the gravitational -wave analysis and how one can use this information to place constraints on the properties of the system. Our simulations suggest that GW190425 is incompatible with an unequal mass binary neutron star merger with a mass ratio q < 0.8 when considering stiff or moderately stiff equations of state if the binary was face on and covered by the observation. Our analysis shows that a detailed observational result for kilonovae will be useful to constrain the mass ratio of binary neutron stars in future events.}, language = {en} } @article{GiegSchianchiDietrichetal.2022, author = {Gieg, Henrique and Schianchi, Federico and Dietrich, Tim and Ujevic, Maximiliano}, title = {Incorporating a Radiative Hydrodynamics Scheme in the Numerical-Relativity Code BAM}, series = {Universe : open access journal}, volume = {8}, journal = {Universe : open access journal}, number = {7}, publisher = {MDPI}, address = {Basel}, issn = {2218-1997}, doi = {10.3390/universe8070370}, pages = {25}, year = {2022}, abstract = {To study binary neutron star systems and to interpret observational data such as gravitational-wave and kilonova signals, one needs an accurate description of the processes that take place during the final stages of the coalescence, for example, through numerical-relativity simulations. In this work, we present an updated version of the numerical-relativity code BAM in order to incorporate nuclear-theory-based equations of state and a simple description of neutrino interactions through a neutrino leakage scheme. Different test simulations, for stars undergoing a neutrino-induced gravitational collapse and for binary neutron stars systems, validate our new implementation. For the binary neutron stars systems, we show that we can evolve stably and accurately distinct microphysical models employing the different equations of state: SFHo, DD2, and the hyperonic BHB Lambda phi. Overall, our test simulations have good agreement with those reported in the literature.}, language = {en} } @article{UjevicRashtiGiegetal.2022, author = {Ujevic, Maximiliano and Rashti, Alireza and Gieg, Henrique Leonhard and Tichy, Wolfgang and Dietrich, Tim}, title = {High-accuracy high-mass-ratio simulations for binary neutron stars and their comparison to existing waveform models}, series = {Physical review : D, Particles, fields, gravitation, and cosmology}, volume = {106}, journal = {Physical review : D, Particles, fields, gravitation, and cosmology}, number = {2}, publisher = {American Physical Society}, address = {College Park}, issn = {2470-0010}, doi = {10.1103/PhysRevD.106.023029}, pages = {10}, year = {2022}, abstract = {The subsequent observing runs of the advanced gravitational-wave detector network will likely provide us with various gravitational-wave observations of binary neutron star systems. For an accurate interpretation of these detections, we need reliable gravitational-wave models. To test and to point out how existing models could be improved, we perform a set of high-resolution numerical relativity simulations for four different physical setups with mass ratios q = 1.25, 1.50, 1.75, 2.00, and total gravitational mass M = 2.7 M???. Each configuration is simulated with five different resolutions to allow a proper error assessment. Overall, we find approximately second-order converging results for the dominant (2,2) mode, but also the subdominant (2,1), (3,3), and (4,4) modes, while generally, the convergence order reduces slightly for an increasing mass ratio. Our simulations allow us to validate waveform models, where we find generally good agreement between state-of-the-art models and our data, and to prove that scaling relations for higher modes currently employed for binary black hole waveform modeling also apply for the tidal contribution. Finally, we also test if the current NRTidal model used to describe tidal effects is a valid description for high-mass-ratio systems. We hope that our simulation results can be used to further improve and test waveform models in preparation for the next observing runs.}, language = {en} }